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The Bulgeless Seyfert/Liner Galaxy Ngc 3367: Disk, Bar, Lopsidedness, and Environment∗

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The Bulgeless Seyfert/Liner Galaxy Ngc 3367: Disk, Bar, Lopsidedness, and Environment∗ The Astronomical Journal, 142:182 (17pp), 2011 December doi:10.1088/0004-6256/142/6/182 C 2011. The American Astronomical Society. All rights reserved. Printed in the U.S.A. THE BULGELESS SEYFERT/LINER GALAXY NGC 3367: DISK, BAR, LOPSIDEDNESS, AND ENVIRONMENT∗ H. M. Hernandez-Toledo´ 1, M. Cano-D´ıaz1,2, O. Valenzuela1, I. Puerari3, J. A Garc´ıa-Barreto1, E. Moreno-D´ıaz1, and H. Bravo-Alfaro4 1 Instituto de Astronom´ıa, Universidad Nacional Autonoma´ de Mexico,´ Apartado Postal 70-264, Mexico´ D. F., 04510, Mexico; [email protected] 2 INAF-Osservatorio Astronomico di Roma, via di Frascati 33, 00040, Monte Porzio Catone, Italy 3 Instituto Nacional de Astrof´ısica, Optica´ y Electronica,´ Calle Luis Enrique Erro 1, 72840, Sta. Maria Tonantzintla, Puebla, Mexico 4 Departamento de Astronoma, Universidad de Guanajuato, Apdo. Postal 144, Guanajuato 36000, Mexico Received 2008 October 15; accepted 2011 March 29; published 2011 October 31 ABSTRACT NGC 3367 is a nearby isolated active galaxy that shows a radio jet, a strong bar, and evidence of lopsidedness. We present a quantitative analysis of the stellar and gaseous structure of the galaxy disk and search for evidence of recent interaction. Our study is based on new UBVRI Hα and JHK images and on archive Hα Fabry–Perot and H i Very Large Array data. From a coupled one-dimensional/two-dimensional GALFIT bulge/bar/disk decomposition a(B/D ∼ 0.07–0.1) exponential pseudobulge is inferred in all the observed bands. A near-infrared (NIR) estimate max = of the bar strength QT (R) 0.44 places NGC 3367 bar among the strongest ones. The asymmetry properties were studied using (1) the optical and NIR concentration–asymmetry–clumpiness indices, (2) the stellar (NIR) and gaseous (Hα,Hi) A1 Fourier mode amplitudes, and (3) the H i-integrated profile and H i mean intensity distribution. While the average stellar component shows asymmetry values close to the average found in the local universe for isolated galaxies, the young stellar component and gas values are largely decoupled showing significantly larger A1 mode amplitudes suggesting that the gas has been recently perturbed and placing NGC 3367 in a global starburst phase. NGC 3367 is devoid of H i gas in the central regions where a significant amount of molecular CO gas exists −2 instead. Our search for (1) faint stellar structures in the outer regions (up to μR ∼ 26 mag arcsec ), (2) (Hα) star-forming satellite galaxies, and (3) regions with different colors (stellar populations) along the disk all failed. Such an absence is interpreted by using results from recent numerical simulations to constrain either a possible tidal event with an LMC like galaxy to some dynamical times in the past or a very low mass but perhaps gas rich recent encounter. We conclude that a cold flow accretion mode (gas and small/dark galaxies) may be responsible for the nuclear activity and peculiar (young stars and gas) morphology regardless of the highly isolated environment. Black hole growth in bulgeless galaxies may be triggered by smooth mass accretion. Key words: galaxies: active – galaxies: general – galaxies: individual (NGC 3367) – galaxies: interactions – galaxies: structure – galaxies: photometry Online-only material: color figures 1. INTRODUCTION Radio observations in NGC 3367 reveal a bipolar synchrotron outflow from the nucleus and two large lobes with a total NGC 3367 is a nearby barred galaxy that is classified as projected extent on the sky (from NE to SW) of 12 kpc, SB(rs)c in the Third Reference Catalog of Bright Galaxies (de resembling a radio galaxy. The axis of the ejected outflow Vaucouleurs et al. 1991, hereafter RC3) and as Sy 2-like, H ii in is highly inclined with respect to the axis of rotation of the Veron-Cetty´ & Veron´ (1986). Mid-infrared Spitzer observations disk (Garc´ıa-Barreto et al. 1998, 2002). Single-dish H i content 9 of NGC 3367 reveal the presence of [Ne v] lines at 14.3 μm of MH i ∼ 7 × 10 M has been reported for this galaxy and 24.3 μm with X-ray luminosity dominated by a power law (Huchtmeier & Richter 1989) and a high fraction of molecular with 2–10 keV luminosities of 2.0 × 1040 erg s−1 (McAlpine gas has been found mostly concentrated in the central 27 (r = 9 et al. 2011). NGC 3367 is located in the field of the Leo 5.7 kpc) M(H 2) = 2.7 × 10 M (Garc´ıa-Barreto et al. 2005). Group but it belongs to the background based on its optical NGC 3367 also shows weak thermal radio continuum emission −1 velocity of vo = 2998 km s and the mean velocity of the Leo (at 4.5 angular resolution) extended throughout the disk (Garc´ıa- I Group = 900 km s−1 (Ferguson & Sandage 1990; Stocke et al. Barreto et al. 1998) and Hα Fabry–Perot observations indicate 1991; Tonry et al. 2001). The closest candidate for a galaxy that its rotation axis lies projected on the disk at a P.A. of 141◦, companion is NGC 3391 at a projected distance of ∼ 563 kpc the N side of that projected line being closer to the observer or 18 optical diameters away (Garc´ıa-Barreto et al. 2003) and (Garc´ıa-Barreto & Rosado 2001). a recent search for isolated galaxies in the local universe based Despite the fact that several properties of NGC 3367 some- on the SDSS has also confirmed that NGC 3367 is an isolated how resemble a gravitational interacting system with another galaxy (Hernandez-Toledo´ et al. 2010). The optical appearance galaxy, there is still no supporting evidence. This is the first of NGC 3367 is dominated by a bright bar and an apparent paper in a series where we present our multi-wavelength data large-scale asymmetry or lopsidedness to the southwest side. and discuss some alternatives to the origin of the observed mor- phology and asymmetries. Our paper is split into two general parts: one describing the observations and the estimate of the ∗ Based on data obtained at the 0.84 m, 1.5 m, and 2.1 m telescopes of the galaxy parameters and the second discussing the interpretation Observatorio Astronomico´ Nacional, San Pedro Martir´ operated by the Instituto de Astronom´ıa, Universidad Nacional Autonoma´ de Mexico.´ of measurements as constraints to the recent dynamical history 1 The Astronomical Journal, 142:182 (17pp), 2011 December Hernandez-Toledo´ et al. in NGC 3367. Specifically, a description of observations and the calibration of the JHK system was performed using the U.K. techniques used in the data reduction are briefly described in Infrared System (Hunt et al. 1998). The sky conditions were Section 2. In Section 3, we present a brief summary of the main almost photometric with a typical seeing FWHM of 2 arcsec. morphological features found in the optical and NIR images. A We also dispose of VLA H i data coming from the NRAO VLA surface photometry analysis is carried out in Section 4, includ- archive, originally obtained in 2001 with the C-configuration. ing (1) an analysis of the surface brightness (SB) and color pro- We produced a full Natural Weighting data cube in order to files; (2) a coupled one-dimensional–two-dimensional (1D–2D) improve the sensitivity. Our final data cube has 63 channels and bulge/disk and bulge/bar/disk decomposition into Sersic,´ Ex- a beam size of 18.7 × 15.6 arcsec. We fully describe the H i data ponential, and Ferrer components. Section 5 presents different reduction in a forthcoming paper (Bravo-Alfaro et al. 2011, in bar properties like interstellar medium (ISM) shocks based on preparation). the dust lane geometry revealed by a B − I color map, a quantifi- cation of the bar strength and length, and a brief discussion of the 3. GENERAL MORPHOLOGY bar nature in terms of the Athanassoula & Misiriotis (2002) mod- The morphology of the galaxy in the optical and NIR bands els. In Section 6, lopsidedness is reviewed from various estima- is shown in Figure 1. Filter-enhanced versions in each band tors, namely, the concentration–asymmetry–clumpiness (here- are also presented (right-hand side), where the sky has been after CAS) parameters in the optical and near-infrared (NIR) = subtracted and the images have been Gaussian-filtered and then bands, the m 0–2 Fourier NIR and Hα amplitudes, and the subtracted from the original image to enhance both internal and Very Large Array (VLA) H i asymmetry from the moment 0 dis- external structures in the form of star-forming regions, structures tribution and the corresponding H i line profile. In Section 7,we embedded into dusty regions, or faint outer details of particular look for (1) evidence of low SB features likely related to a tidal interest for our discussion. origin and (2) the presence of recent galaxy accretion events or The bluer bands highlight a sharp semi-circular outline in the satellite companions in the observed colors. Section 8 presents N–W–S direction. This structure presents a complex pattern of a general discussion of the origin of the disk lopsidedness. We arms at a radius of about 50 arcsec (10 kpc) from the center. use Fabry–Perot Hα and H i VLA data to discuss possible ev- The arms in the inner region almost coalesce to form an internal idence of anisotropic gas accretion and its possible connection ring. Some bright H ii regions are strung along the inner parts to the active galactic nucleus (AGN) activity in NGC 3367. Fi- of two major arms that begin at the ends of the bar, these arms nally, our summary and concluding remarks are presented in = −1 −1 experiencing various levels of winding and branching.
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